For the seismic light curve, we first removed the eclipses using the timestamps from the Kepler Eclipsing Binary Catalog [1]}. The light curves of each quarter were then corrected and stitched together following [2]}. The first step of their method consists of correcting the light curves of each quarter for outliers in the point-to-point deviation function, sudden jumps of the mean value, and drifts. Then, to connect two light curves together at a quarter edge without discontinuity, two methods are considered: first, computing the mean value of the flux, at the end of Q(n) and at the beginning of Q(n+1), and adding or subtracting the difference to the Q(n+1) light curve; and second, fitting the end of Q(n) and beginning of Q(n+1) with first-order polynomials and linking the fits together at the midpoint of the gap between them. Both options are applied and that with the lowest \(\chi ^2\)  is chosen. The light curves we obtained through this process still had long-period trends and periodic gaps owing to instrumental reasons and the eclipse removal. To reduce their impact in the time series, we applied a high-pass filter with a cutoff period of 20 days and filled the gaps using a multiscale discrete cosine transform of an in-painting algorithm [3]}, [4]}.
